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Monte Carlo Simulation of Neutrino Induced EAS

Monte Carlo Simulation of Neutrino Induced EAS. Ofelia Pisanti. In collaboration with Michelangelo Ambrosio, Carla Aramo, Angelo Della Selva, Gennaro Miele, Sergio Pastor, Luigi Rosa. ICRC 2003 – Tsukuba – August 5 th 2003 1/11. Neutrinos as universe messengers.

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Monte Carlo Simulation of Neutrino Induced EAS

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  1. Monte Carlo Simulation of Neutrino Induced EAS Ofelia Pisanti In collaboration with Michelangelo Ambrosio, Carla Aramo, Angelo Della Selva, Gennaro Miele, Sergio Pastor, Luigi Rosa

  2. ICRC 2003 – Tsukuba – August 5th 2003 1/11 Neutrinos as universe messengers Monte Carlo Simulation of Neutrino Induced EAS • observation of EHE n induced showers is very important for getting information on cosmic ray sources in the universe and interactions of n with the matter in presently not accessible energy ranges; • neutrino initiated showers have in principle different signatures from the hadronic ones. But, for extracting physical information from data (Auger) on a more quantitative basis, we need simulations. X. Bertou, P. Billoir, and S. Coutu Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  3. ICRC 2003 – Tsukuba – August 5th 2003 2/11 Neutrino EAS simulation Monte Carlo Simulation of Neutrino Induced EAS The CORSIKA MC is a very powerful tool for the simulation of atmospheric showers for a very large range of the primary energy and is widely used in the community of cosmic rays. Upgrade of Corsika for primaryn induced showers But CORSIKA treats n’s only in a partial way (as not interacting secondary particles produced in  and  decays) How can we implement this option in Corsika? A possibility is to substitute the first interaction with acall to an existing Monte Carlo(HERWIG) which will produce the secondaries of the neutrino interaction. Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  4. ICRC 2003 – Tsukuba – August 5th 2003 3/11 Flow diagram Monte Carlo Simulation of Neutrino Induced EAS Calculate the first interaction point (chi is the interaction length) chi D. Heck, J. Knapp, J.N. Capdevielle, G. Shatz, and T. Thouw CORSIKA 6.014 main program BOX2 CORSIKA intermediate stack  type, energy P. Marchesini, B. Webber, G. Abbiendi, G. Corcella, I. Knowles, S.Moretti, K. Odagiri, P. Richardson, M. Seymour, and L. Stanco FI particles Link routine between CORSIKA and HERWIG NUINT HERWIG 6.4 Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  5. Low energy showers ICRC 2003 – Tsukuba – August 5th 2003 4/11 Monte Carlo Simulation of Neutrino Induced EAS Auger GAP-Note-2003-013 astro-ph/0302602 • Main information: • the fraction of CC events with respect to NC ones is ~ .73 • the lepton carries away an average energy fraction of ~ .70 in e showers, with a “good” probability (~ 73%), ~70% of the energy of the primary  goes to the e.m. component E = 1015 eV  = 70°  = 0° HDPM in m showers ~70% of the energy of the primary  is hidden Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  6. ICRC 2003 – Tsukuba – August 5th 2003 5/11 Outgoing lepton in FI Monte Carlo Simulation of Neutrino Induced EAS The more the energy of the neutrino the larger the fraction of neutrino energy carried by the outgoing lepton. MRST 98 Leading Order PDF’s: x ≥ 10-6; 1.25 GeV2 ≤ Q2 ≤ 107 GeV2 Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  7. Low energy showers ICRC 2003 – Tsukuba – August 5th 2003 6/11 Monte Carlo Simulation of Neutrino Induced EAS Auger GAP-Note-2003-013 astro-ph/0302602 the difference between e and p showers is in the energy of the outgoing electron of the first CC interaction the difference between e and p showers is in the energy of the outgoing electron of the first CC interaction E = 1015 eV  = 70°  = 0° HDPM Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  8. Hadronic models ICRC 2003 – Tsukuba – August 5th 2003 7/11 Monte Carlo Simulation of Neutrino Induced EAS good agreement between different hadronic models HDPM HDPM QGSJET QGSJET E = 1015 eV  = 70°  = 0° Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  9. ICRC 2003 – Tsukuba – August 5th 2003 8/11 Towards higher energies… Monte Carlo Simulation of Neutrino Induced EAS A new .car file has been prepared, which includes a new option for producing the modified CORSIKA Fortran code with primaries. This allows one to choose different hadronic models (QGSJET, DPMJET, NEXUS, …), more reliable at the highest energies of CR spectrum. At the same time, we started a study of the FI with HERWIG, with the aim of singling the main characterizing quantities. Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  10. FI with HERWIG ICRC 2003 – Tsukuba – August 5th 2003 9/11 Monte Carlo Simulation of Neutrino Induced EAS Q2  - q2 = -(k-k’)2 x = Q2/(2 mN) y = / E = (E-El)/ E Q2 = 2 mN E x y 5000 events GRV 98 Leading Order PDF’s: x ≥ 10-9; 0.8 GeV2 ≤ Q2 ≤ 109 GeV2 Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  11. High energy showers ICRC 2003 – Tsukuba – August 5th 2003 10/11 Monte Carlo Simulation of Neutrino Induced EAS • eCC showers very similar to e- ones and more penetrating than p showers • NC first interaction responsible for the suppression of the e profile with respect to the eCC one • extreme suppression of µ profile due to the large fraction of  energy to the outgoing lepton E = 1019 eV  = 70°  = 0° QGSJET E = 1020 eV  = 80°  = 0° QGSJET Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

  12. ICRC 2003 – Tsukuba – August 5th 2003 11/11 Conclusions Monte Carlo Simulation of Neutrino Induced EAS • a new version of CORSIKA for  primaries has been realized and extended to the primary energies of interest for the Auger Observatory • we are carrying on a study of the output of HERWIG, for better understanding the details of the first interaction • the features of neutrino shower longitudinal profiles depend on two competing effects: the amount of  energy to the FI lepton and the number of NC and CC events • future work aims to deeper explore the implications of the different physical assumptions: FI (a different treatment?), PDF’s, hadronic model, charmed particles and  lepton Ofelia Pisanti – http://people.na.infn.it/~astropar/http://www1.na.infn.it/wsubnucl/cosm/auger/index2.html

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